Such super-Eddington models were well reproduced by 2D radiation hydrodynamic
and 2D radiation magneto-hydrodynamic simulations, which take account of viscous and magnetic dissipation, respectively [1]}, [2]}.
They found that the matter can fall onto the black hole with an accretion rate beyond the Eddington limit and the apparent luminosity can exceed the Eddington luminosity because of the photon trapping within the disc. As a result, the supercritical accretion flows show mildly anisotropic and collimated emission and a strong outflow from the disc due to radiation pressure force. The basic difference between their and our work is that we consider the inviscid, low angular momentum flow while they focus on the viscous, high angular momentum flow.
